The nature of the Galactic dSph satellites remains controversial. Do they have extreme M/L? Are they tidally disrupting? Do they contribute significantly to the creation of the halo and halo substructure? Does mass follow light in these Systems? Great insight into these questions will come from high quality radial velocity surveys over large areas, especially for dSph stars well outside the nominal King limiting radii. For most satellites, this work is the realm of 8‐m class echelle spectroscopy, however, the density of suitable stars outside the tidal radius is low enough that little advantage is conferred by most multi‐object spectrographic systems. Worse, the density of good candidates is so low compared to that of foreground Milky Way dwarf stars that clever pre‐filtering is needed to make efficient use of telescopes like SALT for this type of science.